A SIGNIFICANT POPULATION OF CANDIDATE NEW MEMBERS OF THE {rho} OPHIUCHI CLUSTER
- SETI Institute, 189 Bernardo Ave., Suite 100, Mt. View, CA 94043 (United States)
- Physics Department, Utah Valley University, 800 W. University Pkwy., Orem, UT 85058-5999 (United States)
- Infrared Processing and Analysis Center, California Institute of Technology 100-22, Pasadena, CA 91125 (United States)
- Department of Physics and Astronomy, San Francisco State University, 1600 Holloway Ave., San Francisco, CA 94132 (United States)
We present a general method for identifying the pre-main-sequence population of any star-forming region, unbiased with respect to the presence or absence of disks, in contrast to samples selected primarily via their mid-infrared emission from Spitzer surveys. We have applied this technique to a new, deep, wide-field, near-infrared imaging survey of the {rho} Ophiuchi cloud core to search for candidate low-mass members. In conjunction with published Spitzer IRAC photometry and least-squares fits of model spectra (COND, DUSTY, NextGen, and blackbody) to the observed spectral energy distributions, we have identified 948 candidate cloud members within our 90% completeness limits of J = 20.0, H = 20.0, and K{sub s} = 18.50. This population represents a factor of {approx}3 increase in the number of known young stellar objects in the {rho} Ophiuchi cloud. A large fraction of the candidate cluster members (81% {+-} 3%) exhibit infrared excess emission consistent with the presence of disks, thus strengthening the possibility of their being bona fide cloud members. Spectroscopic follow-up will confirm the nature of individual objects, better constrain their parameters, and allow an initial mass function to be derived.
- OSTI ID:
- 22037276
- Journal Information:
- Astrophysical Journal, Vol. 751, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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